For the other new SySt that were not observed by Swift, an estimate of
\(L_{\rm acc}\)  can be derived from the flux recorded in the H\(\alpha \) 
emission. If an emission line forms in an accretion disk, the flux radiated
by the line and the flux emitted by the disk as a whole are related. The
correlation can be tight, with temporal variations in \(L_{\rm acc}\)  that may
be accurately tracked and replicated by \(L\) (H\(\alpha \) ) (cf.
[1]}, their fig. 14).
